Constellation Chart

The Eagle

The Aquila, The Eagle, is a constellation at the East Side of Milky Way. You can see the picture that the constellation adjoins the Milky Way, but Aquila has almost no attractive nebulae nor star clusters. Alpha Aquilae, Altair has a mean of "The Flying Eagle", it's in contrast to Vega, the falling eagle. The star is another main character in the Chinese legend of "Tanabata" with Vega.

Planetary Nebula's In Aquila

B142 - B143

The constellation of Aquila surprisingly includes no Messier objects in spite of being soaked in the summer's Milky Way. But you'll be fascinated with various dark lanes being tangled in the Milky Way through small binoculars, and especially, dark nebulae B142 and B143 (registered in the Barnard's catalogue) are the most striking and vastest ones in them. They're positioned at about 3 degrees NW of Altair (alpha Aquilae), and you can see gamma Aquilae which is a NW neighbor of Altair at the lower left-hand side in the picture. This group of dark nebula looks like a Greek letter of zeta, and is devided into two segments of north (B142) and south (B143) ones.

NGC 6751

This composite color Hubble image of NGC 6751 is a beautiful example of a classic planetary nebula with complex features and was selected to commemorate the tenth anniversary of Hubble in orbit. The colors were chosen to represent the relative temperature of the gas - blue, orange, and red indicating the hottest to coolest gas. Winds and radiation from the intensely hot central star (140,000 degrees Celsius) have apparently created the nebula's streamer-like features. The nebula's actual diameter is approximately 0.8 light-years or about 600 times the size of our solar system. NGC 6751 is 6,500 light-years distant in the constellation Aquila.

NGC2261

It is a fan-shaped cloud of gas and dust which is illuminated by R Monocerotis (R Mon), the bright star at the bottom end of the nebula. Dense condensations of dust near the star cast shadows out into the nebula, and as they move the illumination changes, giving rise to the variations first noted by Hubble. The star itself, lying about 2,500 light-years from Earth, cannot be seen directly, but only through light scattered off of dust particles in the surrounding nebula. R Mon is believed to have a mass of about 10 times that of the Sun, and to have an age of only 300,000 years. There is probably a symmetrical counterpart of the fan-shaped nebula on the southern side of the star, but it is heavily obscured from view by dust lying between this lobe and our line of sight.

HH 32

HH 32 is an excellent example of a "Herbig-Haro object," which is formed when young stars eject jets of material back into interstellar space. This object, about 1,000 light-years from Earth, is somewhat older than Hubble's variable nebula, and the wind from the bright central star has already cleared much of the dust out of the central region, thus exposing the star to direct view. Many young stars, like the central object in HH 32, are surrounded by disks of gas and dust that form as additional material is attracted gravitationally from the surrounding nebula. Material in the disk gradually spirals in toward the star and eventually some of it accretes onto the star, increasing its mass. A fraction of the gas, however, is ejected perpendicularly to the disk at speeds near 200 miles per second, and forms two oppositely directed jets. These jets plow into the surrounding nebula, producing strong shock waves that heat the gas and cause it to glow in the light of hydrogen atoms (green) and sulfur ions (blue), several other atoms and ions, and sometimes radiation from the exciting star that is reflected by the surrounding gas (red). This glow is called a Herbig-Haro object, in honor of astronomers George Herbig and Guillermo Haro, who did much of the early work in this area in the 1950's. The jet on the top side, whose furthest extent is about 0.2 light-year from the star, is pointed more nearly in our direction, while the opposite jet on the bottom lies on the far side of the star and is fainter either because it is partially obscured by dust surrounding the star or because there is much less material in front of the star.

NGC 2346

NGC 2346, in contrast to the first two young objects, is a so-called "planetary nebula," which is ejected from Sun-like stars which are near the ends of their lives. NGC 2346 is remarkable because its central star is known to be actually a very close pair of stars, orbiting each other every 16 days. It is believed that the binary star was originally more widely separated. However, when one component of the binary evolved, expanded in size, and became a red-giant star, it literally swallowed its companion star. The companion star then spiralled downwards inside the red giant, and in the process spewed out gas into a ring around the binary system. Later on, when the hot core of the red giant was exposed, it developed a faster stellar wind, which emerged perpendicularly to the ring and inflated two huge "bubbles." This two-stage process is believed to have resulted in the butterfly-like shape of the nebula. NGC 2346 lies about 2,000 light-years away from us, and is about one-third of a light-year in size.

Galaxies In Aquila

IRAS 19297-0406

The tangled up galaxies, called IRAS 19297-0406, are crammed together in the center of the picture. IRAS 19297-0406 is part of a class of galaxies known as ultraluminous infrared galaxies (ULIRGs). ULIRGs are considered the progenitors of massive elliptical galaxies. ULIRGs glow fiercely in infrared light, appearing 100 times brighter than our Milky Way Galaxy. The large amount of dust in these galaxies produces the brilliant infrared glow. The dust is generated by a firestorm of star birth triggered by the collisions. IRAS 19297-0406 is producing about 200 new Sun-like stars every year . about 100 times more stars than our Milky Way creates. The hotbed of this star formation is the central region [the yellow objects]. This area is swamped in the dust created by the flurry of star formation. The bright blue material surrounding the central region corresponds to the ultraviolet glow of new stars. The ultraviolet light is not obscured by dust. Astronomers believe that this area is creating fewer new stars and therefore not as much dust. The colliding system [yellow and blue regions] has a diameter of about 30,000 light-years, or about half the size of the Milky Way. The tail [faint blue material at left] extends out for another 20,000 light-years. Astronomers used both cameras to witness the flocks of new stars that are forming from the galactic wreckage. NICMOS penetrated the dusty veil that masks the intense star birth in the central region. ACS captured the visible starlight of the colliding system's blue outer region. IRAS 19297-0406 may be similar to the so-called Hickson compact groups . clusters of at least four galaxies in a tight configuration that are isolated from other galaxies. The galaxies are so close together that they lose energy from the relentless pull of gravity. Eventually, they fall into each other and form one massive galaxy.

Planetary Destinations In Aquila

HD 192263

Parent Star: HD 192263 (G0) in the constellation of Aquila is located at a distance of 64.9 Light Years from our Solar system Co-ordinates of Right Ascension: 20 13 59.8451 & Declination: -00 52 00.757. The apparent Magnitude of the star is 8.1. The Inner Edge of Habitability Zone is 0.27 AU & the Outer Edge of Habitability Zone: 0.86 AU and the estimated stellar lifespan of the star is 20282 million years. Orbiting around HD 192263 is planet HD 192263 b the planet is believed to be a Clarified Jovian planet and its exitence has been confirmed. The planets appearance is Blue and cloudless. The Planet orbits out side the habitability zone at 0.15 AU and the estimated radius of the planet is 0.968 Jupiters 1. The planet Orbits around the star every 24.348 1 0.005 Days and was discovered by Santos N., Mayor M., Naef D., Pepe F., Queloz D., Udry S., Burnet M., Revaz Y. in 1999.

HD183263

Parent Star: HD 183263 ( G2 IV ) in the constellation of Aquila is located at a distance of 172.86 Light Years from our Solar system Co-ordinates of Right Ascension: 19 28 24.5727 & Declination: +08 21 28.995. The apparent Magnitude of the star is 7.86. The Inner Edge of Habitability Zone is 0.71 AU & the Outer Edge of Habitability Zone: 2.22 AU and the estimated stellar lifespan of the star is 6243 million years. Orbiting around HD 183263is planet HD 183263 b the planet is believed to be a Water Cloud Jovian, Eccentric planet and its exitence has been confirmed. The planets appearance is white water ice clouds. The Planet is believed to be at Earthlike Temperatures within the habitability zone at 1.52 AU and the estimated radius of the planet is 1.039 Jupiters 1. The planet Orbits around the star every 634.23 Days and was discovered by Marcy et al in the 2005. HD 183263 Planetary System